Stokes I and V observations of magnetic knots using bright CA II K network points as tracers.

Details Stokes I and V observations of magnetic knots using bright CA II K network points as tracers. Stokes I and V observations of magnetic knots using bright CA II K network points as tracers.

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...317..586s&link_type=abstract

Astronomy and Astrophysics, v.317, p.586-593

Astronomy and Astrophysics

Astrophysics

7

Sun: Photosphere, Magnetic Fields

Scientific paper

This paper uses bright Ca II K points as markers for isolated magnetic features in the underlying solar photosphere. Stokes V polarimetry in selected photospheric lines applied to a large number of Ca II K targets yield some average results: These magnetic features are 2 to 3arcsec in diameter, dark at disk center and bright at the limb. Their magnetic field strength is typically 1400Gauss, with the field vertically oriented on average. Their magnetic filling factor is large (=~40%). Our targets share these properties with the magnetic knots introduced by Beckers & Schroeter (1968SPh.....4..142B).We therefore conclude that magnetic knots can be found anywhere on the solar disk and not only near active regions. These features may contribute significantly to the total solar magnetic flux.

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